ABSOLUTE MAGNITUDE CALIBRATION FOR THE W UMA-TYPE SYSTEMS BASED ON HIPPARCOS DATA
ABSOLUTE MAGNITUDE CALIBRATION FOR THE W UMA-TYPE SYSTEMS BASED ON HIPPARCOS DATA
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DOI：
10.1086/134014
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发表时间：
1997-10
影响因子：
3.5
通讯作者：
S. Rucinski;H. Duerbeck
中科院分区：
文献类型：
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作者：
S. Rucinski;H. Duerbeck
使用 40 颗 W UMa 型接触双星（epsilon MV < 0.5）的依巴谷视差数据来推导新的基于 (B-V) 的绝对星等校准，其形式为 MV = MV(log P,B-V)。校准涵盖范围 0.26 < (B-V)0 < 1.14、0.24 < P < 1.15 天和 1.4 < MV < 6.1；它基于视差相对误差（2.7% 至 24%）加权的解决方案。以前的校准并不是基于如此宽的周期和色彩空间，虽然它们已经能够以足够的精度为密切遵循众所周知的周期-色彩关系的系统预测 MV，但新的校准应该能够为更奇特的“外围”接触二元系统提供良好的预测。该校准的主要局限性是地面光度数据质量不足，以及对（B-V）指数的限制，该指数比（V-I）指数对金属丰度效应更敏感；然而，对于局部 W UMa 型系统，金属丰度基本上是未知的。
Hipparcos parallax data for 40 contact binary stars of the W UMa-type (with epsilon MV < 0.5) are used to derive a new, (B-V)-based absolute-magnitude calibration of the form MV = MV(log P,B-V). The calibration covers the ranges 0.26 < (B-V)0 < 1.14, 0.24 < P < 1.15 day, and 1.4 < MV < 6.1; it is based on a solution weighted by relative errors in the parallaxes (2.7% to 24%). Previous calibrations have not been based on such a wide period and color space, and while they have been able to predict MV with sufficient accuracy for systems closely following the well-known period-color relation, the new calibration should be able to give also good predictions for more exotic ''outlying'' contact binary systems. The main limitations of this calibration are the inadequate quality of the ground-based photometric data, and the restriction to the (B-V) index, which is more sensitive to metallicity effects than the (V-I) index; metallicities are, however, basically unknown for the local W UMa-type systems.